AN UPPER LIMIT ON THE MASS OF THE BLACK HOLE IN URSA MINOR DWARF GALAXY
- Instituto de Astronomia, Universidad Nacional Autonoma de Mexico, Ciudad Universitaria, Ap. 70-468, C.P. 04510 Mexico City (Mexico)
The well-established correlations between the mass of massive black holes (BHs) in the nuclei of most studied galaxies and various global properties of their hosting galaxy lend support to the idea that dwarf galaxies and globular clusters could also host a BH in their centers. Direct kinematic detection of BHs in dwarf spheroidal (dSph) galaxies is seriously hindered by the small number of stars inside the gravitational influence region of the BH. The aim of this Letter is to establish an upper dynamical limit on the mass of the putative BH in the Ursa Minor (UMi) dSph galaxy. We present direct N-body simulations of the tidal disruption of the dynamical fossil observed in UMi, with and without a massive BH. We find that the observed substructure is incompatible with the presence of a massive BH of (2-3) x 10{sup 4} M {sub sun} within the core of UMi. These limits are consistent with the extrapolation of the M {sub BH}-{sigma} relation to the M {sub BH} < 10{sup 6} M {sub sun} regime. We also show that the BH may be off-center with respect to the center of symmetry of the whole galaxy.
- OSTI ID:
- 21313036
- Journal Information:
- Astrophysical Journal (Online), Vol. 699, Issue 2; Other Information: DOI: 10.1088/0004-637X/699/2/L113; Country of input: International Atomic Energy Agency (IAEA); ISSN 1538-4357
- Country of Publication:
- United States
- Language:
- English
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